TESS light curves and period changes in low-mass eclipsing binary BB Persei

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F68378271%3A_____%2F25%3A00618794" target="_blank" >RIV/68378271:_____/25:00618794 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/00216208:11320/25:10510257 RIV/00216224:14310/25:00142765 RIV/47813059:19630/25:A0000474

Výsledek na webu

<a href="https://doi.org/10.1016/j.newast.2025.102406" target="_blank" >https://doi.org/10.1016/j.newast.2025.102406</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1016/j.newast.2025.102406" target="_blank" >10.1016/j.newast.2025.102406</a>

Jazyk výsledku

angličtina

Název v původním jazyce

TESS light curves and period changes in low-mass eclipsing binary BB Persei

Popis výsledku v původním jazyce

We present a detailed analysis of the low-mass detached eclipsing binary system BB Persei, which contains two K-type stars in a circular orbit with a short period of 0.4856 d. We used light curves from the Transiting Exoplanet Survey Satellite (Tess), which observed BB Per in five sectors, to determine its photometric properties and a precise orbital ephemeris. The solution of the Tess light curve in Phoebe results in a detached configuration, where the temperature of the primary component was fixed to K according to Lamost, which gives us K for the secondary. The spectral type of the primary component was derived as K0 and the photometric mass ratio was estimated. Slow period changes on the current O-C diagram spanning the past 25 years indicate the presence of a third body orbiting the eclipsing pair with an orbital period of about 22 years. The companion could be a red dwarf of spectral type M6–M7 with a minimal mass of about 0.1 M. The characteristics and temporal variation of the dark region on the surface of the secondary component were estimated.

Název v anglickém jazyce

TESS light curves and period changes in low-mass eclipsing binary BB Persei

Popis výsledku anglicky

We present a detailed analysis of the low-mass detached eclipsing binary system BB Persei, which contains two K-type stars in a circular orbit with a short period of 0.4856 d. We used light curves from the Transiting Exoplanet Survey Satellite (Tess), which observed BB Per in five sectors, to determine its photometric properties and a precise orbital ephemeris. The solution of the Tess light curve in Phoebe results in a detached configuration, where the temperature of the primary component was fixed to K according to Lamost, which gives us K for the secondary. The spectral type of the primary component was derived as K0 and the photometric mass ratio was estimated. Slow period changes on the current O-C diagram spanning the past 25 years indicate the presence of a third body orbiting the eclipsing pair with an orbital period of about 22 years. The companion could be a red dwarf of spectral type M6–M7 with a minimal mass of about 0.1 M. The characteristics and temporal variation of the dark region on the surface of the secondary component were estimated.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10303 - Particles and field physics

Projekt

<a href="/cs/project/GN24-10608O" target="_blank" >GN24-10608O: Výzkum populací symbiotických systémů a příbuzných dvojhvězd s červenými obry</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2025

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

New Astronomy

ISSN

1384-1076

e-ISSN

1384-1092

Svazek periodika

119

Číslo periodika v rámci svazku

Oct

Stát vydavatele periodika

NL - Nizozemsko

Počet stran výsledku

7

Strana od-do

102406

Kód UT WoS článku

001454813900001

EID výsledku v databázi Scopus

2-s2.0-105000645397